To this end, we proposed to use both MUSTANG-2 and NIKA2 in order to map the SZ signal of the most SZ luminous cluster in the sky, RX J1347\(-\) 1145 at \(z=0.45\) , at an angular resolution \(<18\)  arcsec and on scales of few arcmin at 90, 150, and 260 GHz. The MUSTANG-2 observations were realized at the Green Bank Telescope during the instrument commissioning phase for 2 hours. The NIKA2 observations have been conducted in the context of an Open Time program for a total of 24 hours. The top panels of Fig. REF  show the MUSTANG-2 map (left) obtained with the MIDAS software [1]} and the NIKA2 maps (middle and right) realized from a preliminary analysis based on the procedure described in [2]}. All three maps have been smoothed at an effective resolution of 20 arcsec. The extended SZ signal is detected at \(>3\sigma \)  on a sky area of about \(2\times 1.5~\mathrm {arcmin}^2\) . We detect a strong positive signal in the cluster core at 260 GHz due to a radio AGN. This signal compensates the negative SZ signal at 90 GHz and 150 GHz. We also detect a sub-millimeter galaxy to the south-west of the cluster, which also alters its morphology at 150 GHz. As a preliminary test, we measured the average SZ surface brightness in a region (red rectangle in Fig. REF ) where a shock has been detected in previous analyses [3]} and far enough from the detected point sources to minimize their contamination. The measurements are shown as purple points in the lower panel of Fig. REF . We use the SZpack software [4]} in order to compute the expected SZ spectrum for ICM temperatures of 1 keV (dashed blue line) and 20 keV (red line), assuming a null bulk velocity along the line of sightNote that having three SZ constraints will also enable fitting the kinetic SZ component in the total SZ signal.. While changing the value of the Compton parameter \(y_{tSZ}\)  allows us to fit the data at 90 GHz and 150 GHz in both cases, we are able to exclude an ICM temperature of 1 keV at more than \(5\sigma \)  in the shock region based on the measurement realized at 260 GHz. A careful characterization of the point source, cosmic infrared background, and kSZ contamination using Herschel and spectroscopic data will allow us to produce the first ICM temperature map of a galaxy cluster based on the resolved detection of the rSZ effect.
